[1]} performed hydrodynamics simulations for specific stellar and planetary parameters, but being isothermal, their simulations can be rescaled (approximately; see their Section 3.2.3) to apply to other values.
For PDS 70 b, using a gas surface density from [2]} and scaling to the stellar mass of \({M_{\star }}\approx 0.8~{M_\odot }\) , they considered masses of \(M_{\mathrm {p}}=0.5\) –2.4 \(M_{\mathrm {J}}\)  and accretion rates \(\dot{M} =(2\) –\(3)\times 10^{-8}~M_{\mathrm {J}}\,\mathrm {yr}^{-1}\) . This \(\dot{M}\)  is dictated by the rescaling of their simulations through (E. Sanchis 2021, pers. comm.)
\(\dot{M}^{\prime } = \dot{M} \left(\frac{a}{a^{\prime }}\right)^3\frac{\Sigma _1^{\prime }}{\Sigma _1}\sqrt{\frac{{M_{\star }}^{\prime }}{{M_{\star }}}},\) 
